{
    "count": 4,
    "next": null,
    "previous": null,
    "results": [
        {
            "id": 5103,
            "url": "https://svs.gsfc.nasa.gov/5103/",
            "result_type": "Visualization",
            "release_date": "2023-05-24T00:00:00-04:00",
            "title": "Dancing on the Limb - May 1, 2023",
            "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.A large loop of solar plasma executes some interesting long-lived (15 hours in this series) gyrations on the lower solar limb. || ",
            "hits": 22
        },
        {
            "id": 5102,
            "url": "https://svs.gsfc.nasa.gov/5102/",
            "result_type": "Visualization",
            "release_date": "2023-05-11T12:00:00-04:00",
            "title": "When Coronal Holes are Smiling.... - October 26, 2022",
            "description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.In another example of pareidolia (Wikipedia) we have what appears to be a smiling face in the SDO/AIA 193 Angstrom filters formed by the arrangement of the darker coronal holes.  Coronal holes form at the footpoints of open magnetic field lines which form a 'fast track' for the outflowing solar wind.  These 'open' field lines do not connect back to the Sun but instead reach out to the heliopause and interstellar medium.  The fast solar wind has an average speed of about 750 kilometers per second, compared to the slow solar wind with speeds from 300 to 500 kilometers per second.For comparison, we include the same time frame from the AIA 171 Angstrom filter where the 'face' is much less pronounced. || ",
            "hits": 78
        },
        {
            "id": 4854,
            "url": "https://svs.gsfc.nasa.gov/4854/",
            "result_type": "Visualization",
            "release_date": "2020-09-15T10:00:00-04:00",
            "title": "Coronal Holes at Solar Minimum and Solar Maximum",
            "description": "A sample of solar coronal holes around the time of the maximum of sunspot activity (April 2014).  Note the polar regions are devoid of coronal holes but a large hole appears in the southern hemisphere. || CoronalHoleMax_AIA193_00150_print.jpg (1024x1024) [173.1 KB] || CoronalHoleMax_AIA193_00150_searchweb.png (320x180) [89.6 KB] || CoronalHoleMax_AIA193_00150_thm.png (80x40) [7.4 KB] || CoronalHoleMax_AIA193_2048p30.mp4 (2048x2048) [61.7 MB] || CoronalHoleMax_AIA193_2048p30.webm (2048x2048) [2.9 MB] || AIA193-Time (4096x4096) [64.0 KB] || AIA193-Frames (4096x4096) [64.0 KB] || CoronalHoleMax_Timestamp (600x100) [64.0 KB] || ",
            "hits": 176
        },
        {
            "id": 4101,
            "url": "https://svs.gsfc.nasa.gov/4101/",
            "result_type": "Visualization",
            "release_date": "2013-09-20T10:00:00-04:00",
            "title": "August 2013: SDO Observes Large Coronal Hole",
            "description": "On the Sun, coronal holes represent regions where the solar magnetic field does not connect back to the Sun. In these cases, the magnetic field guides the charged particles of the solar wind into distant space, forming the fast solar wind. || ",
            "hits": 27
        }
    ]
}